VERS UNE ASTRONOMIE NEUTRINO AVEC IceCube+ANTARES+KM3NeT DAMIEN DORNIC (CPPM) CFR Cos: Meeting de la communauté de recherche sur le rayonnement cosmique!! APC - 26-28 mars 2018
NEUTRINO AS COSMIC MESSENGER Neutrinos: smoking gun for cosmic-ray interactions! 3 GeV 1 TeV: atmospheric neutrinos, dark matter! 100 GeV - 30 TeV: various galactic (TeV gamma) sources! 30 TeV 3 PeV: IceCube signal (astrophysical flux) ORCA ANTARES ARCA 2
HE NEUTRINO PRODUCTION The sources of HE ν are not necessary the sources of UHECR 3
HE NEUTRINO FLUXES } Cf O. Martineau s talk 4
HE NEUTRINO DETECTORS 5
HE NEUTRINO DETECTORS ANTARES BAIKAL GVD KM3NeT ORCA ARCA IceCube Gen-2 GNN: Global Neutrino Network linked all HE neutrino telescopes + provide framework for regular combined meetings and combined analysis 6
ALL-FLAVOR NEUTRINO TOPOLOGIES Direction: Gal. srcs: 0.2 o at 10TeV [0.4 o for ANTARES] Extra-gal. srcs: 0.1 o at 100TeV [0.3 o for ANTARES] Energy: 0.27 in Log10(E) Not to scale Vertex: 6-8m (long), 0.5m (perp) Direction: ~1.5 o [3 o for ANTARES] Energy: 5% 7
LARGELY DOMINATED BY ATM BKG To have better discovery potential: - Have the lowest angular precision (tracks) - Have the lowest background contamination (cascades) - Search for time+space-correlations 8
THE ICECUBE SIGNAL 6 year HESE analysis (ICRC 2017) 80(+2) events Bkg: 15.6+11.4-3.9 atm nu + 25.2+/-7.3 atm mu Hemipshere North and South Eth: 60 TeV 8 year upgoing muon Eth: 200 TeV Eevent >5 PeV! Significance: Significance: 6.5 sigma Spectra: E-2.92(+0.33-0.29) 6.7 sigma Spectra: E -2.19(+/-0.10) Indication of a break in spectrum? (energy threshold different) Indication of galactic and extra-galactic components? (different hemispheres) 9
THE ICECUBE SIGNAL Last update for the starting track analysis 10
THE ICECUBE SIGNAL Last update for the starting track analysis Indication of a break in spectrum? (energy threshold different) Indication of galactic and extra-galactic components? (different hemispheres) 11
ANTARES DIFFUSE RESULTS Track events Cascade events Preliminary All-sky / All-flavor neutrino search Look for excess above a given Eth 9 (7) yrs of data for tracks (cascades) Bkg expectation Signal exceptation => Small excess (not significant) Nb events measured Track 13+/-3 3 19 Shower 5+/-2 1.5 7 Preliminary 12
KM3NeT: DIFFUSE FLUX All-sky KM3NeT/ARCA is expected to observe the IC signal in less than 1 yr. Galactic plane Precise characterization (spectral shape, flavor composition, anisotropy) Excellent sensitivity in the galactic plane: identify gal/extra-gal components? 13
γ-ν-rc DIFFUSE FLUXES Energy density of neutrinos in the non-thermal Universe is the same or higher as that in Fermi gamma-rays. Common sources? Fermi/LAT γ-ray flux dominated by AGN/blazars (~ 85%) 14
POPULATION STUDIES Blazar space correlation GRB time/space correlation (862 2LAC blazars) Contribution max of the 2LAC blazars < 27% (10 TeV - 2 PeV), assuming equal weighting among blazars and single power-law with γ = 2.5. 7% of neutrino signal assuming ν flux γ-ray flux (correlation with 2FHL: < few % of the IC flux) Astrophysical Journal 835 (2017) 1 (1172 GRBs - benchmark parameters) arxiv:1702.06868 15
POPULATION STUDIES Blazar space correlation GRB time/space correlation (862 2LAC blazars) Contribution max of the 2LAC blazars < 27% (10 TeV - 2 PeV), assuming equal weighting among blazars and single power-law with γ = 2.5. BUT, neutrinos originate from a larger volume 50% of blazars not identified Sources transparent to high energy gamma rays may not have the target density to produce neutrinos (GRB?) Hidden sources? How to identify these sources? Neutrino only, neutrino+x-ray? 7% of neutrino signal assuming ν flux γ-ray flux (correlation with 2FHL: < few % of the IC flux) Astrophysical Journal 835 (2017) 1 (1172 GRBs - benchmark parameters) arxiv:1702.06868 16
GALACTIC DIFFUSE FLUX 17
IC NEUTRINO SKYMAP Where are the PeV γ-rays together with PeV neutrinos? 18
IC NEUTRINO SKYMAP 19
LOOKING FOR POINT-SOURCES IceCube (7 yrs - tracks) ANTARES ANTARES+IceCube 20
KM3NeT: POINT-SOURCE Generic source KM3NeT/ARCA is expected to have more than one order of magnitude better sensitivity than IC in the Southern sky. Due to the quite good angular resolution for cascade events, the point-source search is also very efficient. Expected better performances for the transient neutrino sources (GRB, AGN ) 21
KM3NeT: POINT-SOURCE Specific galactic sources γ ν flux conversion: With reasonable 100% hadronic models, large probabilities to observe individual neutrino sources in the Galactic Plane 22
LOOKING FOR VARIABLE SOURCES No correlation with GRB, FRB Few hints with blazars (nothing significant) One hint with SN Ic (IC160427) Connection ν-γ-uhecr Resconi et al 2017, 2.9 sigma correlation with sub-sample of HBLs, IC nu and Auger UHECR IceCube- Big Bird PKS B1424-418 23
KM3NeT MULTI-MESSENGER PROGRAMS Follow-up of neutrino alerts Joint sub-threshold analysis CTA LSST KM3NeT SVOM HAWC SKA LIGO/VIRGO Follow-up of EM/GW alerts Offline time/space correlation search with catalogues (GRB, AGN, XRB, SN, FRB ) TAROT 24
IC170922 / TXS 0506+056? (signalness ~ 50%) (E proxy ~ 120 TeV) Distance to TXS 0506+056? Paiano et al. (2018):the 10.4m Gran Telescopio Canarias, an optical spectroscopy z = 0.3365 +/- 0.0010 25
ν PREDICTIONS FOR AGN For AGN, very few groups are developing lepto-hadronic models: Produce very high energy neutrinos >1 PeV 3C279 PKS 2155-304 PKS B1424-418 Richter, Spanier, arxiv:1802.08820 Zech, Cerruti, Mazin, A&A 602 (2017) 25 Gao, Paul, Winter, ApJ. 843 (2017) 2 +Winter et al, Böttcher et al., Petropoulou et al., Zdziarski et al., Is it possible to produce intermediate energy neutrinos [1-50 TeV]? In which condition? Correlation with 100 MeV - 10 GeV or 100 GeV - 10 TeV γ-rays? 26
NEUTRINO FROM GRB170817/GW170817? Biehl, Heinze, Winter, arxiv:1712.00449 ANTARES, IceCube, Auger, LIGO/VIRGO, ApJ, 850 (2017) L35 Kimura, Murase, Mészaros & Kiuchi, ApJL, 848 (2017) L4 27 For this special event, very different computations. Need to be ready for the next interesting events Standard GRBs seem to not be efficient neutrino producers. Do we still have a chance to detect individual GRB? Which parameters?
MODELISATION To improve discovery potential, need to know where/when to look for neutrino association: correlation with TeV γ-ray?, GeV γ-ray?, X-ray? Radio flares? For galactic sources, the sensitivities of future telescopes (ARCA/ Gen-2) are closed to the model predictions, need also more sophisticated models (lepto-hadronic, better implementation of microphysics). We have few hints that transient/variable sources could brighter HE neutrino sources (blazars, SN ), need to have time-dependent hadronic models (arxiv:1410.5380) Most of the neutrino predictions are at very high or ultra high energies, need models for intermediate energy range [50 GeV - 50 TeV] One strength of IceCube is that theoreticians are part of the collaboration. This interaction is quite weak in our collaboration. [It is free to be observator in the KM3NeT Collaboration] 28
Summary Multi-messenger astronomy era! (GW + neutrino) Diffuse flux of cosmic neutrinos observed by IceCube Higher level of hadronic activity in the non-thermal universe than previously thought Sources remain to be identified. Hints are pointing in MM analyses. We are quite closed! Exciting times ahead! KM3NeT: phased approach to next-generation neutrino telescope ARCA (KM3NeT-It) for HE neutrino astronomy (tracks & showers) ORCA (KM3NeT-Fr) for measurement of neutrino mass hierarchy First strings performing well!!! Start to implement the multi-messenger programs in KM3NeT for both ORCA and ARCA based on the successful experience of ANTARES. The follow-up of gravitational waves have worked very well and the community is organizing itself to get an even better follow-up of GW events. Neutrinos are a bit left in this structurant process. Need to think more in a multi-messenger manner rather than separated the messenger. 29
KM3NeT IN FRANCE APC IPHC In France, 4 groups: APC, CPPM, IPHC, Subatech (+LAM, MIO observator) ~ 15 permanent physicians 50/50 between low and high energy activities Subatech CPPM (LAM) KM3NeT is a multi-purpose experiment, we have access to all ORCA/ARCA data. KM3NeT neutrino data are proprietary but become public after a latency of 2 years after the data taking (except neutrino alerts). It is free to be observator in the Collaboration [only sign paper with contributions, no shift] On KM3NeT, we have the responsibilities for: Neutrino oscillation group: PMNS oscillation parameters, neutrino mass hierachy, CP phase Multi-messager group: time-dependent searches for GRB, AGN, FRB, realtime alerts, MM analysis (GW, IC, UHECR ), MeV neutrino SNe 30
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